WINDS FROM T-TAURI STARS .2. BALMER LINE-PROFILES FOR INNER DISK WINDS

Balmer line profiles have been calculated using escape probability methods for T Tauri wind models with non-spherically symmetric geometry. The wind is assumed to originate in the inner regions of an accretion disk surrounding the T Tauri star, and flows outward in a "cone" geometry. We consider two types of wind models, both with monotonically increasing expansion velocities as a function of radial distance. For flows with large turbulent velocities, such as the high-frequency Alfven wave-driven wind models, the effect of cone geometry is to increase the blue wing emission, and to move the absorption reversal close to line center. This type of model can provide good agreement with observed H-alpha line profiles of some T Tauri stars. However, even in cone geometry turbulent wind models still tend to produce too much blueshifted absorption in H-beta and H-gamma. We have also calculated line profiles for a wind model rotating with the same angular velocity as the inner disk. The Balmer lines of this model are significantly broader than observed in most objects, suggesting that the observed emission lines do not arise in a region rotating at Keplerian velocity. Both turbulent and rotating wind models have difficulties explaining the centrally peaked emission line profiles often observed. Thus, the wind models considered here do not provide very satisfactory explanations of the Balmer line profiles of many T Tauri stars.